A few final words are in order to explain the non-detection of GaSS 1-11 and
1-12 in X-rays in our shallow observations. The upper limit to their flux
is about 0.01\(\times \)  the flux Mk16 recorded from SU Lyn during their Swift observations. Those observations of SU Lyn were obtained during an
exceptionally bright state of the accretion disk (cf.
Fig. REF  and the discussion at the end of
Section ), while the flux at other times (when the H\(\alpha \) 
shown by SU Lyn is much weaker and more similar in appearance to that
revealed by GALAH spectra for our sample of 33 acc-SySt) was just 1/10
of that (cf. [1]}). There are two other factors playing
against GaSS 1-11 and 1-12. The most important is the distance. SU Lyn is
just 0.65 kpc away, while GaSS 1-11 and 1-12 are respectively at 6.6
and 4.6 kpc distance according to Gaia \(e\) DR3 parallaxes, corresponding to
dilution factors of 100 and 50. In addition, SU Lyn is seen face-on, while
the unknown orbital inclination of GaSS 1-11 and 1-12 introduces a reduction
in flux proportional to \(\cos i\)  and a further reduction for limb-darkening
reasons. Considering all factors together, it is no wonder that GaSS 1-11
and 1-12 fell below the X–ray detection threshold of snapshot ToO with Swift.
